Radial profiles of the mean magnitude of the magnetic field, ⟨B⟩, in different regions for cluster II. The upper panel shows the profiles at 200 kyr, and the lower panels shows them at 390 kyr. The profiles were obtained by averaging over 10 000 randomly drawn line-outs. Points are only plotted where at least 10% of line-outs pass through the indicated region. ⟨B⟩ scales approximately as r⁻¹ in the supersonic cluster wind. The hump in the stellar winds profile close to 0.6 pc stems from magnetic stars and is traced by a hump in the subsonic core medium. This indicates that wind material from magnetic stars significantly increases the magnetisation of the bulk.